NGC 3137

In this article we are going to delve into NGC 3137, exploring its impact, importance and relevance in today's society. NGC 3137 has been the subject of interest and debate for many years, and its influence can be seen in different areas of daily life. Throughout this article we will examine different perspectives and opinions on NGC 3137, with the aim of providing a complete and balanced view of this topic. Additionally, we will discuss how NGC 3137 has evolved over time and how it continues to shape our lives today. Without a doubt, NGC 3137 is a fascinating topic that deserves our attention and reflection, and we are sure that this article will give you an enriching insight into it.

NGC 3137
NGC 3137 imaged by PanSTARRS
Observation data (J2000 epoch)
ConstellationAntlia
Right ascension10h 09m 07.3775s[1]
Declination−29° 03′ 50.486″[1]
Redshift0.003683 ± 0.000002 [1]
Heliocentric radial velocity1,104 ± 1 km/s[1]
Distance52.6 ± 9.1 Mly (16.1 ± 2.8 Mpc)[1]
Group or clusterNGC 3175 Group
Apparent magnitude (V)11.5[2]
Characteristics
TypeSA(s)d [1]
Size~138,000 ly (42.2 kpc) (estimated)[1]
Apparent size (V)6.3′ × 2.2′[1]
Other designations
ESO 435- G 047, AM 1006-284, UGCA 203, MCG -05-24-024, PGC 29530[1]

NGC 3137 is a spiral galaxy in the constellation Antlia. The galaxy lies about 50 million light years away from Earth, which means, given its apparent dimensions, that NGC 3137 is approximately 140,000 light years across.[1] It was discovered by John Herschel on February 5, 1837.[3]

NGC 3137 has a pretty bright nucleus. The spiral pattern is similar with NGC 3621 and the Pinwheel Galaxy and features many knots.[4] The morphological classification of this galaxy is SA(s)d,[1] which indicates the galaxy doesn't have a bar (SA), lacks an inner ring structure (s), and has loosely wound spiral arms (d). A star is superposed 0.3 arcminutes from the centre.[4] The galaxy is seen at an inclination of about 70°.[5]

The star formation rate of the galaxy is estimated to be 0.5 M☉ per year based on the CO(2-1) radio emission detected by the Atacama Large Millimeter Array. The total hydrogen mass of the galaxy is estimated to be 109.68 M☉. The stellar mass of the galaxy is comparable, at 109.88 M☉.[5] In the centre of the galaxy lies a supermassive black hole, whose mass is estimated to be 107.78 ± 0.20 (38 - 95 millions) M☉, based on the pitch angle of the spiral arms.[6]

NGC 3137 is a member of the NGC 3175 Group.[7] It is one of the two large spirals of the group, the other being NGC 3175.[8] Other members of the group include NGC 3113, and NGC 3125.[9]

See also

References

  1. ^ a b c d e f g h i j k "Results for object NGC 3137". NASA/IPAC Extragalactic Database. NASA and Caltech. Retrieved 2 March 2025.
  2. ^ "Revised NGC Data for NGC 3137". spider.seds.org. Retrieved 30 March 2024.
  3. ^ Seligman, Courtney. "NGC 3137 (= PGC 29530)". Celestial Atlas. Retrieved 19 November 2018.
  4. ^ a b Corwin, H. G.; de Vaucouleurs, A.; de Vaucouleurs, G (1985) Southern Galaxy Catalogue. University of Texas
  5. ^ a b Leroy, Adam K.; et al. (1 December 2021). "PHANGS–ALMA: Arcsecond CO(2–1) Imaging of Nearby Star-forming Galaxies". The Astrophysical Journal Supplement Series. 257 (2): 43. arXiv:2104.07739. Bibcode:2021ApJS..257...43L. doi:10.3847/1538-4365/ac17f3.
  6. ^ Davis, Benjamin L.; Berrier, Joel C.; Johns, Lucas; Shields, Douglas W.; Hartley, Matthew T.; Kennefick, Daniel; Kennefick, Julia; Seigar, Marc S.; Lacy, Claud H. S. (20 June 2014). "The Black Hole Mass Function Derived from Local Spiral Galaxies". The Astrophysical Journal. 789 (2): 124. arXiv:1405.5876. Bibcode:2014ApJ...789..124D. doi:10.1088/0004-637X/789/2/124. S2CID 119302157.
  7. ^ Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv:1011.6277. Bibcode:2011MNRAS.412.2498M. doi:10.1111/j.1365-2966.2010.18071.x. S2CID 119194025. Retrieved 1 February 2025.
  8. ^ Kondapally, Rohit; Russell, George A; Conselice, Christopher J; Penny, Samantha J (1 December 2018). "Faint satellite population of the NGC-3175 Group – a Local Group analogue". Monthly Notices of the Royal Astronomical Society. 481 (2): 1759–1773. arXiv:1808.09020. doi:10.1093/mnras/sty2333.
  9. ^ Garcia, A. M. (1 July 1993). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47–90. Bibcode:1993A&AS..100...47G. ISSN 0365-0138.
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